From the cosmological observations, it is clear that the fluid variables (shear stress, expansion scalar, vorticity tensor etc.) defining the kinematics of stellar configuration have substantial effects on its stability. Herrera et al. [1]} provided in-depth analysis of the physical meaning of scalar functions by taking into account a dissipative spherical fluid distribution with the inclusion of electromagnetic force along with the effects of cosmological constant. They investigated the part played by such scalar functions and also studied the physical outcomes. Letelier [2]} propounded a two-perfect-fluid model by taking into account anisotropic fluid and investigated the energy-momentum tensor associated with the model with focus on the stress tensor. A comparison between the Einstein's equations of the propounded model and a complex scalar field without mass is also carried out. Herrera and Santos [3]} extended the criteria of jeans instability to the stellar configurations having anisotropic stresses and found that instabilities may occur for the masses smaller than the corresponding jeans mass of local isotropic matter distribution. Herrera et al. [4]} analyzed instability for a spherically symmetric matter with anisotropic pressure collapsing adiabatically following restriction of zero expansion scalar by taking Newtonian and post-Newtonian regimes under consideration. They found that the instability range can be evaluated using pressure anisotropy in the fluid and radial depiction of energy density independent of stiffness.
